The detection of gravitational-wave (GW) signals from astrophysical systems [1]} has ushered in a new era in astronomy [2]}, [3]}, allowing the study of systems previously invisible. The current generation of GW interferometric detectors are sensitive enough to allow a confident candidate event about once per week [4]}, [5]}. Increasing the sensitivity of the detectors is important not only to increase the detection rate but also to improve the signal to noise ratio and sky localization of events, allowing for a more precise probing of the properties of nuclear matter in neutron stars [6]} and of the fundamental physics of gravitation and general relativity [7]}.
